Spatially Resolved Outflows In a Seyfert Galaxy at z = 2.39 3 3 3 1 1 2 3 2 3 3 1 Travis Fischer , Jane Rigby , Guillaume Mahler , Michael Gladders , Keren Sharon , Michael3 Florian3 , Steve Kraemer4, Matt Bayliss5, Håkon Dahle6, L. Felipe Barrientos7, Eva Wuyts8, Traci L. Johnson3 3 3 1665, NASA's Goddard Space Flight Center, Greenbelt, MD, United States 2University of Michigan 3University of Chicago 4Catholic University of America 5MIT 6University of Oslo 7Pontifical Catholic University of Chile 8Max Planck Institute for Extraterrestrial Physics

We present spatially resolved analysis of rest-frame optical and UV imaging and spectroscopy for a lensed galaxy at z = 2.39 that hosts an active galactic nucleus. Proximity to a natural guide star has enabled high signal-to-noise VLT SINFONI + adaptive optics observations of rest-frame optical diagnostic emission lines, which exhibit an underlying broad component with FWHM ∼700 km/s in both the Balmer and forbidden lines. Measured line ratios place the outflow robustly in the region of the ionization diagnostic diagrams associated with AGN. We compare the spatial extent and morphology of the Lyα, UV and dust-corrected Hα emission, and disentangle the effects of star formation and AGN ionization on each tracer. This unique opportunity — combining gravitational lensing, AO guiding, redshift, and AGN activity — allow a complete and magnified view of three main tracers of the physical conditions and structure of the interstellar medium in a star-forming galaxy hosting a weak AGN at cosmic noon.

Left: From our strong lensing model, we find the lensing critical line, which separates regions of different image multiplicities, lies directly over the center of the arc of SGAS 0033, such that the north and south ends of the arc are reflections of one another and sample roughly half of the fully imaged galaxy. Right: Source plane reconstruction of the arc shows SGAS 0033 as it would have been seen without a lens. 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K-band continuum centroid is depicted by a cross. measured NLR gas mass of 7.4 x 10 M☉, we calculate a mass E outflow rate of Ṁ = 0.55 M☉ yr-1 . F555W F814W Star formation rate (SFR) F105W Hα luminosity measured from the non-AGN ionized gas is converted to a SFR using the Kennicutt (1998) relation and adjusted to the initial mass function from Charbrier (2003). Bottom circle: HST WFC3 F555W/F814W/F105W composite Measuring the source plane Hα luminosities north and south image of the lensed Sloan Giant Arcs Survey (SGAS) galaxy, of the lensing critical line , we find SFRs of 22.8 M☉ yr-1 and SGAS2-0033. SINFONI observations of the target lensed arc -1 are shown approximately by the green box. The bright source 70.7 M☉ yr , respectively. Measuring the individual, extended to the southeast is a star, which was used as the natural guide Hα emission knots offset from the continuum peak, we star for SINFONI adaptive optics. The bright source to the measure a SFR of 2 - 5 M☉ yr-1. southwest is a star, which was used as the natural guide star for SINFONI adaptive optics. Above left: BPT diagram of individual spaniel measurements using the high-redshift classification from Kewley+ (2013). Grey We have analyzed spatially-resolved, rest-frame UV / optical imaging and spectroscopy of a Seyfert AGN at Lyα vs Hα Flux points are single component fits, red points are two-component We find that the Lyα-emitting gas is Hα + [N II] fits. Above right: Separating the two-component fits z∼2 for the first time. Our major findings are as follows: most prominent between, not into narrow (green) and broad (blue) components shows that the 1) Observed AGN-ionized outflows have a maximum cospatial with, the brightest knots of Lyα broad component is AGN ionized. Larger points represent extent of ~100 pc. We calculate a mass outflow rate over Hα that reside over the AGN and likely spectrum from 0.5” x 0.5” binned region over the location of the this distances of Ṁ = 0.55 M⊙ yr−1. The corresponding star-forming regions. This discrepancy broad component gas. between the morphology of Lyα and Below: Gaussian fits to the 0.5” x 0.5” binned spectrum and ratio of outflow power to bolometric luminosity is Hα is similar to what has been resultant fluxes in both the observed image plane and the exceedingly low, log(Ė/Lbol) = -3.76, suggesting that the reported in local starburst galaxies reconstructed source plane. AGN provides little impact on the host galaxy. (Ostlin et al. 2009; Hayes et al. 2013) 2) SGAS 0033 is also exhibits a SFR on the order of 10s

Lyα vs Hα Velocity Profile of solar masses per year, which greatly exceeds the We also compare the spectral Lyα AGN mass outflow rate. As such, the current state of the signatures of Lyα and Hα, with Lyα Hα + [N II] AGN in SGAS 0033 would be unlikely to quench star- emission obtained from longslit MagE formation within the galaxy. observations as detailed in Rigby+ 2018. The observed velocity structure 3) AGN outflows have little effect on Lyα structure of Lyα in comparison to Balmer compared to similar galaxies not hosting AGN. emission is typical in studies of green 4) Faint emission-line signatures of AGN combined with pea galaxies (Yang et al. 2017; strong star formation makes detecting AGN at z∼2 Orlitova et al. 2018). extremely difficult without gravitational lensing.